GHASP：螺旋星系和不规则星系的Hα运动学巡天-- IX。NIR、恒星和重子Tully-Fisher关系
GHASP: an Hα kinematic survey of spiral and irregular galaxies -- IX. The NIR, stellar and baryonic Tully-Fisher relations
摘要：
我们研究了，第一次，近红外，恒星和重子Tully-Fisher关系的场星系的样本从一个均匀的法布里-珀罗样本的星系（GHASP调查）。GHASP相对于其他样本的主要优点是，最大旋转速度是从2D速度场估计的，避免了对星系倾角和位置角的假设。通过结合这些数据与2 MASS测光，光学颜色，HI质量和不同的质光比估计，我们发现一个斜率为4.48 \pm 0.38和3.64 \pm 0.28恒星和重子Tully-Fisher关系，分别。我们发现，当使用不同的质光比配方时，这些值不会发生显着变化。我们还指出，第一次，上升的旋转曲线，以及不对称的旋转曲线表现出更大的分散在塔利-费舍尔关系比平坦的或对称的。利用星系的重子质量和光学半径，我们发现该样本中所有星系的表面重子质量密度几乎是常数。在这项研究中，我们还强调了在M（H，K）\sim-20的近红外塔利-费舍尔关系的中断的存在，我们证实，晚型星系提出了更高的总重子质量比早型螺旋，这表明超新星反馈实际上是一个重要的问题，在晚型螺旋。由于GHASP星系的Tully-Fisher关系具有良好的样本选择标准和数据分析的均匀性，因此它可以作为研究其他环境和高红移下Tully-Fisher关系的参考。
英文摘要：
We studied, for the first time, the near infrared, stellar and baryonic Tully-Fisher relations for a sample of field galaxies taken from an homogeneous Fabry-Perot sample of galaxies (the GHASP survey). The main advantage of GHASP over other samples is that maximum rotational velocities were estimated from 2D velocity fields, avoiding assumptions about the inclination and position angle of the galaxies. By combining these data with 2MASS photometry, optical colors, HI masses and different mass-to-light ratio estimators, we found a slope of 4.48\pm0.38 and 3.64\pm0.28 for the stellar and baryonic Tully-Fisher relation, respectively. We found that these values do not change significantly when different mass-to-light ratios recipes were used. We also point out, for the first time, that rising rotation curves as well as asymmetric rotation curves show a larger dispersion in the Tully-Fisher relation than flat ones or than symmetric ones. Using the baryonic mass and the optical radius of galaxies, we found that the surface baryonic mass density is almost constant for all the galaxies of this sample. In this study we also emphasize the presence of a break in the NIR Tully-Fisher relation at M(H,K)\sim-20 and we confirm that late-type galaxies present higher total-to-baryonic mass ratios than early-type spirals, suggesting that supernova feedback is actually an important issue in late-type spirals. Due to the well defined sample selection criteria and the homogeneity of the data analysis, the Tully-Fisher relation for GHASP galaxies can be used as a reference for the study of this relation in other environments and at higher redshifts.
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